Article
Bootstrapped Newtonian Cosmology and the Cosmological Constant Problem
Roberto Casadio1,2,*,† and Andrea Giusti3,†
Citation: Casadio, R.; Giusti, A.
Bootstrapped Newtonian Cosmology and the Cosmological Constant Problem. Symmetry 2021, 13, 358.
https://doi.org/10.3390/sym13020358
Academic Editor: Kazuharu Bamba and Yi-Fu Cai
Received: 14 January 2021 Accepted: 19 February 2021 Published: 22 February 2021
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1 Dipartimento di Fisica e Astronomia “A. Righi”, Università di Bologna, via Irnerio 46, I-40126 Bologna, Italy
2 I.N.F.N., Sezione di Bologna, IS - FLAG, via B. Pichat 6/2, I-40127 Bologna, Italy
3 Department of Physics and Astronomy, Bishop’s University, 2600 College Street, Sherbrooke, QC J1M 1Z7, Canada; agiusti@ubishops.ca
* Correspondence: casadio@bo.infn.it
† These authors contributed equally to this work.
Abstract:Bootstrapped Newtonian gravity was developed with the purpose of estimating the impact of quantum physics in the nonlinear regime of the gravitational interaction, akin to corpuscular models of black holes and inflation. In this work, we set the ground for extending the bootstrapped Newtonian picture to cosmological spaces. We further discuss how such models of quantum cosmol- ogy can lead to a natural solution to the cosmological constant problem.
Keywords:dark energy; quantum gravity; cosmological constant
1. Introduction
The standard model of the present Universe, often referred to as theΛ-Cold Dark Matter (ΛCDM) model, allows us to include the current accelerated expansion of the Universe, confirmed by type I supernovae surveys [1], in the broader scheme of general relativity. However, this is carried out at the price of adding an ad hoc cosmological constant termΛ in the Einstein field equations or by assuming the existence of an exotic fluid, dubbed dark energy, of which the pressure p and energy density ρ are such that ρ+p≈0. Throughout the work we set the speed of light c=1, while we express Newton’s constant GN = `p/mpand Planck’s constant ¯h= `pmpin terms of the Planck length`p and the Planck mass mp. Further, we use'to denote that two quantities are equal up to order-one multiplicative factors.
Corpuscular gravity [2–4] is a quantum description based on the classicalization scheme [5] applied to the gravitational interaction. In some detail, the ultraviolet incom- pleteness of the Einstein–Hilbert gravity is conjectured to be cured by the formation of extended bound states of a large number of soft (off-shell) gravitons in very energetic processes (for interesting cases with a few gravitons involved see Reference [6]). These gravitons are prone to escape the bound state by quantum depletion, since they are very weakly coupled with each other and to other fields, but the large occupation endows the collective quantum state with a quasi-classical behaviour. According to this paradigm, a black hole of mass M is understood as a marginally bound state of N'M2/m2poff-shell gravitons of typical momentum eG'mp/√
N interacting with each other with an effective coupling αG ' 1/N. Since the collective coupling N αG ' 1, the bound state cannot hold on to its constituents and will slowly lose components by the process of quantum depletion. The depletion of constituent gravitons represents the quantum precursor of the semiclassical Hawking evaporation as a consequence of the softness of the constituents and combinatorics. In fact, the master equation of the Hawking emission is recovered in the semiclassical limit of the theory, i.e., for N→∞ and`p→0, with the length scale
L=√
N`p (1)
Symmetry 2021, 13, 358. https://doi.org/10.3390/sym13020358 https://www.mdpi.com/journal/symmetry
and ¯h kept fixed and finite. In the language of Bose–Einstein condensates, a “corpuscular”
black hole is a condensate of gravitons on the verge of a quantum phase transition, which re- mains at the critical point throughout the evaporation process, up until the quantum break-time of the system. This “quantum criticality” provides nearly-gapless Bogoliubov modes (with energy gap∆e∼1/N) accounting for the entropy of the black hole. A similar scenario can be derived from the Hamiltonian approach to gravity for the gravitational collapse of compact spherically symmetric distributions of matter [7]. Further, it is worth noting that this peculiar quantum description of black holes is strictly intertwined with the generalised uncertainty principle [8] and it has interesting implications for black-hole echoes [9].
Other space-times equipped with horizons have been studied within this scenario.
In particular, one can apply arguments similar to the one above for black holes to the de Sitter space [3,10–14], embedding inflation and the late-time evolution of the Universe within a single theoretical paradigm. This corpuscular picture of the Universe further allows one to explain the dark matter phenomenology as the response of the cosmological condensate of gravitons, responsible for the quasi-de Sitter behaviour at a large scale, to the local presence of impurities, i.e., galaxies and (possibly) clusters of galaxies. Addition- ally, the corpuscular Hamiltonian approach [7] for cosmological spaces provides a quantum exclusion principle for the de Sitter space [3,10] and phantom energy [15].
In a nutshell, bootstrapped Newtonian gravity [16–20] is an approach aimed at pro- viding a more detailed field-theoretic realisation for the quantum corpuscular theory of (spherically symmetric) compact sources. This approach has at its core the idea that, if quantum effects were negligible, starting from a field theory reproducing Newton’s gravity, one should be able to recover general relativistic configurations by reconstructing (leading-order) non-linearities out of the coupling of each constituent graviton with the collective state. However, quantum effects are not assumed to be negligible and depar- tures from general relativity are therefore expected (see, e.g., References [4,16,17] for more details). This procedure represents, to some extent, an analogue of Deser’s conjecture that the Einstein–Hilbert action in the vacuum should be obtained from a Fierz–Pauli Lagrangian for spin 2 fields in Minksowski space-time by adding suitable self-coupling terms [21,22]. Our approach instead focuses on the interplay between non-linearities and quantum physics in order to determine possible quantum corrections to the predictions of general relativity for compact but large self-gravitating systems in the strong field regime, for which the matter content is also far from the quantum vacuum.
In this work, we lay the basis for an extension of the bootstrapped Newtonian picture to cosmology, where the much simpler homogenous and isotropic spaces allow us to analyse also higher order terms. Furthermore, we show how this novel paradigm provides a natural solution to the cosmological constant problem.
2. Corpuscular Models
Let us start from the assumption that matter and the corpuscular state of gravitons together must reproduce the Einstein equations. In particular, we will focus on the Hamil- tonian constraint corresponding to the time-reparameterisation invariance of the theory (the Hamiltonian constraint also plays the role of ensuring total energy conservation in a suitable sense)
HM+HG=0 , (2)
where HM is the matter energy and HG the analogue quantity for the graviton state.
We recall that local gravity being attractive in general implies that HG≤0, although this is not true for the graviton self-interaction [7,16].
2.1. Corpuscular De Sitter and Black Holes
The corpuscular models of gravity of References [2–4] were first introduced for de- scribing black holes but are perhaps easier to obtain in cosmology, as the two systems share
a fundamental “critical” condition. In order to have the de Sitter space-time in general relativity, one must assume the existence of a cosmological constant term, or vacuum energy density ρ, so that the Friedman equation (for spatially flat Universe) reads
3 ˙a a
2
=8 π GNρ. (3)
Upon integrating on the volume inside the Hubble radius L= a
˙a, (4)
we obtain
L'GNL3ρ'GNM . (5)
This relation looks like the expression of the horizon radius for a black hole of ADM mass M and is the reason it was conjectured that the de Sitter space-time could likewise be described as a condensate of gravitons [3].
One can describe the ideal corpuscular model as a condensate of N (soft off-shell) gravitons of typical Compton length equal to L in Equation (1). Then, since M=N eGand eG=¯h/L, one can infer that
M= N`pmp
L =√
N mp, (6)
in agreement with Equation (5). This shows that for a macroscopic black hole, or de Sitter universe, one needs a huge number N 1. Since the above corpuscular relations are more realistically expected to hold only approximately, we will assume that the energy M is exactly given in terms of the fixed number of gravitons N by Equation (6), whereas the Compton length of the gravitons denoted by L henceforth can be (slightly) different from the Hubble value in Equation (1), which we will denote with LN = GNM = √
N`p. We thus write the Compton length as
L=ξ−1
√N`p≡ξ−1LN, (7)
where ξ is a positive constant of order one which will play a significant role in the following analysis. In particular, we anticipate that we will find L& LN, that is ξ.1, so that the gravitons must spread outside the Hubble radius LN.
2.2. “Post-Newtonian” Corpuscular Models
Let us refine the above corpuscular description. In References [7,16], it was shown that the maximal packing condition, which yields the scaling relations (7) for a black hole actually follow from the energy balance (2) when matter becomes totally negligible. If HM=0, one is left with
HG=UN+UPN =0 , (8)
where HGis given by the sum of the negative (of course, we must assume the gravitational interaction is attractive and it is then important to keep track of minus signs in the following expressions) Newtonian energy [7]
UN 'N eG' −N`pmp
L ' −`pM2
L mp , (9)
and the positive “post-Newtonian” contribution [7]
UPN 'N
√N`2pmp
L2 ' `2pM3
L2m2p . (10)
One therefore immediately recovers the scaling relation (7) from Equation (8), regard- less of whether L is the horizon radius of the de Sitter universe or of a black hole.
3. Bootstrapped Newtonian Series Let us now note that
UN' −
√N`p
L
!
M= −ξ M, (11)
where ξ was introduced in Equation (7), and
UPN' −ξ UN' LNM
L2 , (12)
where we remark that L is the Compton length of gravitons associated with either the horizon radius LNof the de Sitter universe or of a black hole. This leads us to conjecture that the complete form of the gravitational Hamiltonian to all orders in the ξ expansion is given by
HG'M
∑
∞ n=1gn(−ξ)n, (13)
where we notice that g1 ' g2 ' 1 and the alternating signs above are precisely due to the attractiveness of gravity. This sort of expansion is strictly related to the argument of resurgence in QFT. In particular, the values of gnshould arise directly from this argument (see, e.g., Reference [23]).
For a black hole, a matter contribution is needed and we cannot have HG = 0.
In particular, assuming the scaling relation (7), we note in passing that Equation (13) would reproduce the Newtonian expectation (we recall that the horizon radius can in fact be interpreted in terms of Newtonian gravity as the size of a source with escape velocity equal to the speed of light), that is
HG'UN, (14)
for gn 'e ξ1−n/n!(e−1)(Note that in this “Newtonian” case, the condition g1'g2'1 does not hold.) Equation (2) then yields HM ' UN with this expression of the coeffi- cients gn.
One more naive observation is that the typical momentum of the constituent gravitons scales as 1/L which, in turn, is related to the spectral representation of the differential operator d/dr. Hence, one could view the exponential Equation (13) as the realisation of the black hole quantum state in infinite derivative gravity [24]. More precisely, one can see that the Schwarzschild metric (or quantum modifications thereof, and perhaps quantum general relativity as a whole), should be recovered as an infinite derivative theory in flat space-time (where the corpuscular picture is naturally formulated). Again, this is in line with bootstrapped Newtonian gravity [16,17] and Deser’s works [21,22].
From now on we shall focus on pure gravity and cosmology, for which Equation (13) is more suitable. Let us then try to keep the analysis of Equation (13) as general as possible.
We only require gn >0 in the series (13) and the “on-shell” condition
HG(L) =0 for L= ¯L=ξ−1LN, (15)
with ξ >0 (and of order one) in the scaling relation (7). First of all, the series (13) converges provided the coefficients gnsatisfy the inequality
gn+1<ξ−1gn. (16)
Note that, for our purpose, convergence is strictly required only for L= ¯L. Assuming however the series converges for L at least in a neighbourhood of ¯L, the Hamiltonian HG
must be a smooth function of L around ¯L, that is
∂kHG
∂Lk L= ¯L
= M
∑
∞ n=1gn ∂k
∂Lk
−LN L
n L= ¯L
, (17)
for some integers 1 ≤ k ≤ K. Approaching the cosmological (or black hole) horizon, the contributions of nonlinear order of the theory will become of the same order of the Newtonian one, signalling the beginning of the full non-perturbative regime of gravity.
This suggests that, not only g1 ' g2 ' 1 but also gn = O(1) for all n ≥ 1 (when L approaches LN), which is indeed consistent with Equation (8). Putting together this observation with the condition in Equation (16), the convergence of the above series requires ξ to be smaller of anO(1)constant, which depends on the specific behaviour of the sequence of coefficients gn. We remark that we always assume that the energy M is fixed by the number of gravitons according to Equation (6) and it therefore does not depend on the Compton length L (again for values around LN). We then expect to obtain (slightly) more restrictive conditions for the coefficients gn.
At this point, it is more interesting to consider other quantities of physical interest, and employ their relations with HG, in order to obtain further conditions on the coefficients gn. For instance, we know that the pressure p= −ρin pure de Sitter space-time. From
p= 1
4 π L2
∂HG
∂L L= ¯L
= M
4 π ¯L2
∑
∞ n=1gn
∂
∂L
−LN L
n L= ¯L
= − M 4 π ¯L3
∑
∞ n=1n gn(−ξ)n, (18)
where we again used Equation (6). On considering the first two terms only (n=1, 2) and HG=0 up to the same order, that is g1=ξ g2, one finds
p= −M g2ξ
2
4 π ¯L3 = −g2mpξ
5
4 π`3pN . (19)
From Equations (5), (6) and (15), we find
ρ= M
4 π ¯L3 = mpξ
3
4 π`3pN, (20)
so that p= −ρimplies
g2=ξ−2=g21. (21)
Upon replacing this solution into Equation (13), we obtain the (slightly) off-shell Hamiltonian
HG(L) =M
−ξ−1
√N`p L
! +ξ−2
√N`p L
!2
+
∑
∞ n=3gn −
√N`p L
!n
, (22)
where the higher-order terms should progressively capture all the non-linearities of the quantum theory of gravity. By looking at Equation (22), we can furthermore conjecture
that gn 'ξ−n, but the precise values of such coefficients of interest to us will have to entail the specific features of the actual quantum state of the Universe. The precise determination of the gn for the observable Universe hence requires further investigation, as they will necessarily depend on the actual matter distribution and time evolution, which led to the present state.
In particular, since our Universe is not empty now, we can employ a more general equation of state for the purpose of improving our estimates of the coefficients gn. In fact, we can easily generalise the above picture for any equation of state of the form
p= −ω ρ, (23)
where 0<ω≤1 is a constant. This yields g2
ω =ξ−2 = g
2 1
ω2. (24)
We can then conjecture that gn 'ω ξ−n. Note that the pure dust case p=0 turns out to be rather peculiar in this scenario. Indeed, there are two possible configurations that allow Equation (18) to reduce to p=0: (i) gn =0,∀n≥2, i.e., the purely Newtonian case, in agreement with the Newtonian derivation of the Friedmann equation (3); (ii) ξ = 0, which implies N →0, thus reducing to Minkowski space.
We can finally notice that, upon employing the present value for the Hubble size of the Universe, that is LN' ¯L'1027m, Equation (20) yields the correct order of magnitude for the present total energy density
ρ= M
4 π ¯L3 '10−28 kg
m3 , (25)
without any further assumptions. From Equation (20) and the definition (7) we can addi- tionally estimate the observed value
ξ=
4 π ρ `p mpL2N
1/3
'0.9<1 , (26)
which implies that the Compton length of the background gravitons L>LN, as anticipated.
Equation (24) can then be implemented to infer the equation of state parameter ω'ξ g1' 0.9 g1and g2'g1/ξ'1.1 g1, where we again recall that g1'1. In fact, all of these final estimates are consistent with our previous assumption that the coefficients gn=O(1).
The above (somewhat preliminary) analysis shows that the apparently unnatural small value of the cosmological constant is indeed consistent with the quantum state of the observable Universe obtained from the bootstrapped Newtonian approach (see also References [3,25]). Moreover, a detailed comparison with cosmological measurements can be employed in order to determine the fine details of the quantum state of gravitons forming the background of the present quasi-de Sitter Universe. Of course, one would need to consider the time evolution of the Universe from the surface of the last scattering in order to determine the particle horizon. We leave such a question for further developments.
4. Concluding Remarks
Inspired by the corpuscular theory of gravity, in which the (matter empty) de Sitter Universe is described by a bound state of gravitons, we have shown how one can express the gravitational Hamiltonian HGfor a cosmological space to all “post-Newtonian” orders as the Newtonian energy of the leading order UN multiplied by a power series in the quantity ξ = LN/L, where L is the Compton length of the bound gravitons and LN is the Hubble radius of the Universe determined by its (vacuum) energy M. In other words, similarly to Deser’s classical argument [21,22], one can reconstruct the full quantum Hamiltonian of cosmology by supplying (“bootstrapping”) the Newtonian potential energy
with the energies due to particle self-interactions within the marginally bound state. At the fundamental level, this further suggests that general relativity might be recovered as an infinite derivative field theory on a flat space-time, although quantum corrections are naturally expected to introduce deviations from the classical configurations, which will result in different values of the coefficients in the “post-Newtonian” expansion (13).
A crucial role in our analysis is played by the parameter ξ, which measures the (slight) departure from the ideal corpuscular relation L = LN. A functional behaviour for the coefficients of the bootstrapped Newtonian expansion of HGin powers of ξ−1 around the ideal de Sitter case with ω =1 was then obtained in Equation (22). In order to accommodate for our non-empty observable Universe, we allowed for a more general equation of state. In particular, if one sets the radius LN'L of the cosmological horizon to the present size of the Universe, the corpuscular Hamiltonian constraint of cosmology yields an energy density that matches the observed one associated with the cosmological constant provided the parameter ξ '0.9<1. This implies that L&LNand the gravitons spread slightly beyond the measured Hubble size. Hence, this prediction for the vacuum energy density coming solely from the observed size of the Universe and the corpuscular quantum description of cosmological spaces can arguably be regarded as leading to a natural solution of the cosmological constant problem.
Author Contributions: All authors have contributed equally, read and agreed to the published version of the manuscript.
Funding:This research received no external funding.
Institutional Review Board Statement:Not applicable for studies not involving humans or animals.
Informed Consent Statement:Not applicable for studies not involving humans.
Data Availability Statement:Not applicable for studies not reporting any data.
Acknowledgments:R.C. is partially supported by the INFN grant FLAG. A.G. is supported by the Natural Sciences and Engineering Research Council of Canada (Grant No. 2016-03803 to V. Faraoni) and by Bishop’s University. This work has been carried out in the framework of activities of the Italian National Group for Mathematical Physics (Gruppo Nazionale per la Fisica Matematica (GNFM), Istituto Nazionale di Alta Matematica (INdAM)) and COST action Cantata.
Conflicts of Interest:The authors declare no conflict of interest.
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